J/A+A/674/A64ivo://CDS.VizieR/J/A+A/674/A64doi:10.26093/cds/vizier.36740064CDSLe N.Karska A.Figueira M.Sewilo M.Mirocha A.Fischer C.,Kazmierczak-Barthel M.Klein R.Gawronski M.Koprowski M.Kowalczyk K.,Fischer W.J.Menten K.M.Wyrowski F.Koenig C.Kristensen L.E.2025-08-26T20:00:56Z2023-06-01T13:51:55ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fryoung-stellar-objectsinfrared-photometryinfrared-astronomyspectroscopyinterstellar-masersFar-infrared line emission provides key information about the gas cooling and heating due to shocks and UV radiation associated with the early stages of sta r formation. Gas cooling via far-infrared lines might depend, however, on metallicity. We aim to quantify the far-infrared line emission, determine the spatial distribution of CO rotational temperature, ultraviolet (UV) radiation field, and H2 number density toward the embedded cluster Gy 3-7 in the CMa-l224 star-forming region, whose metallicity is expected to be intermediate between the Large Magellanic Cloud and the Solar neighborhood. By comparing the total luminosities of CO and [OI] toward Gy 3-7 with values found for low- and high-mass protostars extending over a broad range of metallicities, we also aim to identify the possible effects of metallicity on the far-infrared line cooling within our Galaxy. We study SOFIA/FIFI-LS spectra of Gy 3-7 covering several CO transitions from J=14-13 to 31-30, the OH doublet at 79um, the [OI] 63.2 and 145.5um, and the [CII] 158um lines. The field-of-view covers a 2'x1' region with a resolution of ~7"-18". The spatial extent of CO high-J (Jup>=14) emission resembles that of the elongated 160 um continuum emission detected with Herschel, but its peaks are offset from the positions of the dense cores. The [OI] lines at 63.2um and 145.5um follow a similar pattern, but their peaks are found closer to the positions of the cores. CO transitions from J=14-13 to J=16-15 are detected throughout the cluster and show a median rotational temperature of 170+/-30K on Boltzmann diagrams. Comparison to other protostars observed with Herschel shows a good agreement with intermediate-mass sources in the inner Galaxy. Assuming an origin of the [OI] and high-J CO emission in UV-irradiated C-shocks, we obtain pre-shock H_2_ number densities of 10^4^-10^5^cm^-3^ and UV radiation field strengths of 0.1-10 Habing fields (G0). Far-IR line observations reveal on-going star formation in Gy 3-7, dominated by intermediate-mass Class 0/I young stellar objects. The ratio of molecular-to-atomic far-IR line emission shows a decreasing trend with bolometric luminosities of the protostars. However, it does not indicate that the low-metallicity has an impact on the line cooling in Gy 3-7.2023A&A...674A..64Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A64CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/674/A64https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/674/A64http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/674/A64https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/674/A64https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/674/A64http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/674/A64GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/674/A64/list (List of datacubes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/674/A64/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/674/A64/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/674/A64/list?GETtext/xml+votable180.050000true107.36451-10.84030.005555555555555556Cone search capability for table J/A+A/674/A64/tablec1 (*Multi-wavelength photometry of YSO candidates in the IRAS field.)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/674/A64/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/674/A64/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/674/A64/tablec1?GETtext/xml+votable180.050000true107.32592-10.827720.0055555555555555566/216453.972892068905477e-22 1.7003137259100215e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/674/A64?format=asciiInfrareddefaultJ/A+A/674/A64/listList of datacubesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintNzNumber of slicesmeta.numberintObs.dateObservation datestime.epoch;obsnullablebWAVELower value of wavelength interval0.1nmem.wldoubleBWAVEUpper value of wavelength interval0.1nmem.wldoubledWAVEWavelength resolution0.1nmspect.resolutiondoublesizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitscharJ/A+A/674/A64/table2CO rotational temperature, the number of emitting molecules, and total line luminosities of CO and [OI] lines toward dense cores in Gy 3-7 and IM YSOs from Matuszak et al. (2015A&A...578A..20M)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroup[AB] Group (1)meta.idcharSourceSource namemeta.id;meta.maincharTrotCO rotational temperature (2)Kphys.temperatureinte_TrotUncertainty of rotational temperature (2)Kstat.errorintlogNtotBase-10 logarithm of total number of emitting molecules (2)meta.numberfloate_logNtotUncertainty of logNtot (2)stat.errorfloatLCOTotal CO luminosity in warm component (3)msolLumphys.luminosityfloate_LCOUncertainty of LCO (3)msolLumstat.errorfloatLOI63Luminosity of [O I] 63 um linemsolLumphys.luminosityfloate_LOI63Uncertainty of LOI63msolLumstat.errorfloatLOI145Luminosity of [O I] 145 um linemsolLumphys.luminosityfloate_LOI145Uncertainty of LOI145msolLumstat.errorfloatJ/A+A/674/A64/table4Physical parameters for a subset of YSO candidates with at least 5 photometric data pointsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource identification numbermeta.id;meta.mainintModelSetModel Set name (G1)meta.id;stat.fitcharClassYSO class as determined from the SED fitting (see Sect. 4.5)src.classcharR*Stellar radiussolRadphys.size.radiusfloatT*Stellar temperatureKphys.temperatureintL*Stellar LuminositysolLumphys.luminosityfloatM*? Stellar mass (1)solMassphys.massintnullableAge? Stellar age (1)Myrtime.agefloatnullableNoteNote for YSO (2)meta.notecharJ/A+A/674/A64/tablea1Parameters of the 22 GHz H2O maser lines detected toward CMa l224 with RT4recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroup[AB] Group (1)meta.idcharObs.dateObservation datetime.epoch;obscharVpCentral velocity of of the water maser linekm/sphys.veloc;em.wl.centralfloate_VpUncertainty of Vpkm/sstat.errorfloatSpFlux density peakJyphot.flux.density;em.radiofloate_SpUncertainty of SpJystat.error;src.spTypefloatFWHMFWHMkm/sphys.angSizefloate_FWHMUncertainty of FWHMkm/sstat.error;phys.angSizefloatintSdVIntegrated flux densityJy.km/sphot.flux.density;em.radiofloate_intSdVUncertainty of intSdVJy.km/sstat.errorfloatJ/A+A/674/A64/tableb1Flux SOFIA FIFI-LS toward the two dense cores within a beam size of 20"recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelengthumem.wlfloatFAFlux at core A1e-16W.m**-2phot.flux.density;em.radiofloate_FAUncertainty of FA1e-16W.m**-2stat.errorfloatFB? Flux at core B1e-16W.m**-2phot.flux.density;em.radiofloatnullablee_FB? Uncertainty of FB1e-16W.m**-2stat.errorfloatnullableJ/A+A/674/A64/tablec1*Multi-wavelength photometry of YSO candidates in the IRAS field.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource identification numbermeta.id;meta.mainintRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainSJ? 2MASS J fluxmJyphot.flux.density;em.IR.Jfloatnullablee_SJ? 2MASS J flux errormJystat.errorfloatnullableSH2MASS H fluxmJyphot.flux.density;em.IR.Hfloate_SH2MASS H flux errormJystat.errorfloatSKs2MASS Ks fluxmJyphot.mag;em.IR.Kfloate_SKs2MASS Ks flux errormJystat.errorfloatS3.6? IRAC 3.6um fluxmJyphot.mag;em.IR.3-4umfloatnullablee_S3.6? IRAC 3.6um flux errormJystat.errorfloatnullableS4.5? IRAC 4.5um fluxmJyphot.mag;em.IR.4-8umfloatnullablee_S4.5? IRAC 4.5um flux errormJystat.errorfloatnullableSW1? AllWISE 3.4um (W1) fluxmJyphot.mag;em.IR.3-4umfloatnullablee_SW1? AllWISE 3.4um (W1) flux errormJystat.errorfloatnullableSW2? AllWISE 4.6um (W2) fluxmJyphot.mag;em.IR.4-8umfloatnullablee_SW2? AllWISE 4.6um (W2) flux errormJystat.errorfloatnullableSW3? AllWISE 12um (W3) fluxmJyphot.flux.density;em.IR.8-15umfloatnullablee_SW3? AllWISE 12um (W3) flux errormJystat.errorfloatnullableSW4? AllWISE 22um (W4) fluxmJyphot.flux.density;em.IR.15-30umdoublenullablee_SW4? AllWISE 22um (W4) flux errormJystat.errorfloatnullableS70? PACS 70um fluxJyphot.flux.density;em.IR.30-60umfloatnullablee_S70? PACS 70um flux errorJystat.errorfloatnullableS160? PACS 160um fluxJyphot.flux.density;em.mm.1500-3000GHzfloatnullablee_S160? PACS 160um flux errorJystat.errorfloatnullableS250? SPIRE 250um fluxJyphot.flux.density;em.mm.750-1500GHzintnullablee_S250? SPIRE 250um flux errorJystat.errorfloatnullableS350? SPIRE 350um fluxJyphot.flux.density;em.mm.750-1500GHzfloatnullablee_S350? SPIRE 350um flux errorJystat.errorfloatnullableS500? SPIRE 500um fluxJyphot.flux.density;em.mm.400-750GHzfloatnullablee_S500? SPIRE 500um flux errorJystat.errorfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullableJ/A+A/674/A64/tabled1CO rotational temperature and number of emitting molecules for HM YSOs, derived by fitting the rotational diagram of CO using all and only four available CO transitionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSourceSource namemeta.id;meta.maincharTrot4Rotational temperatures calculated using 4 CO transitions with Jup = (14, 16, 17, 22)Kphys.temperatureinte_Trot4Uncertainty in Trot4Kstat.errorintTrotaRotational temperatures calculated using all detected CO transitions, data is adopted from Karska et al. (2014A&A...562A..45K).Kphys.temperatureinte_TrotaUncertainty in TrotaKstat.errorintDiffThe relative difference between Trot4 and Trota is taken as |1-Trot4/Trota|*100%stat.fit.paramfloatJ/A+A/674/A64/tabled2Far-IR line cooling luminosity of the sample in the Milky Way (MW), LMC, and SMC used to compare with results of this studySourceSource namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroup[ABCD] Group (1)meta.idcharDDistancekpcpos.distancefloate_D? Distance errorkpcstat.errorfloatnullabler_DReference of distances (G2)meta.ref;pos.frameintRGC? Galactocentric radius (2)kpcpos.distance;pos.galactocentricfloatnullableZMetallicity compared to Zsun (3)phys.abund.ZfloatlogLbolBased-10 logarithm of bolometric to solar luminosity ratiolog(solLum)phys.luminosityfloatr_logLbolReference of logLbol (G2)meta.ref;pos.frameintLCOLuminosty of CO in warm component (4)0.01solLumphys.luminosityfloate_LCO? Uncertainty of LCO0.01solLumstat.errorfloatnullableLOILuminosity of [OI] line (5)0.01solLumphys.luminosityfloate_LOI? Uncertainty of LOI0.01solLumstat.errorfloatnullableLratioLuminosity ratio of CO to [OI]phys.luminosity;arith.ratiofloate_Lratio? Uncertainty of Lratiostat.errorfloatnullablerefLlineReference of the line luminosities (G2)meta.id;spect.lineint